An optimised gravitational wave follow-up strategy with the Australian Square Kilometre Array Pathfinder
An optimised gravitational wave follow-up strategy with the Australian Square Kilometre Array Pathfinder
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DOI：
10.1017/pasa.2019.9
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发表时间：
2019-03
影响因子：
6.3
通讯作者：
D. Dobie;T. Murphy;D. Kaplan;S. Ghosh;K. Bannister;R. Hunstead
中科院分区：
文献类型：
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作者：
D. Dobie;T. Murphy;D. Kaplan;S. Ghosh;K. Bannister;R. Hunstead
先进激光干涉引力波天文台和先进室女座引力波探测器探测到的中子星星合并，以及随后探测到的电磁对应物，开启了瞬变天文学的新时代。随着先进激光干涉仪引力波天文台和先进处女座探测器的升级以及日本和印度即将上线的新探测器，中子星星合并将在未来以更高的速度被探测到，从2019年初开始的O3观测运行开始。这些合并的电磁辐射的检测提供了有关合并参数的重要信息，并允许独立测量哈勃常数。澳大利亚平方公里阵列探路者预计将于2019年初全面投入使用，其30度2的视野将使我们能够快速调查大面积的天空。在这项工作中，我们探索的前景与澳大利亚平方公里阵列探路者探测中子星星合并的即时和长期的无线电发射，并确定一个观测策略，优化使用望远镜的时间。我们研究了不同的策略，以瓷砖的天空望远镜指向，以检测无线电同行有限的观测时间，使用475模拟引力波事件。我们的研究结果表明，与覆盖整个局部化的天真策略相比，即使在达到相同的总概率覆盖时，观察效率也有显着提高。
Abstract The detection of a neutron star merger by the Advanced Laser Interferometer Gravitational-Wave Observatory and Advanced Virgo gravitational wave detectors, and the subsequent detection of an electromagnetic counterpart have opened a new era of transient astronomy. With upgrades to the Advanced Laser Interferometer Gravitational-Wave Observatory and Advanced Virgo detectors and new detectors coming online in Japan and India, neutron star mergers will be detected at a higher rate in the future, starting with the O3 observing run which will begin in early 2019. The detection of electromagnetic emission from these mergers provides vital information about merger parameters and allows independent measurement of the Hubble constant. The Australian Square Kilometre Array Pathfinder is expected to become fully operational in early 2019, and its 30 deg2 field of view will enable us to rapidly survey large areas of sky. In this work we explore prospects for detecting both prompt and long-term radio emission from neutron star mergers with Australian Square Kilometre Array Pathfinder and determine an observing strategy that optimises the use of telescope time. We investigate different strategies to tile the sky with telescope pointings in order to detect radio counterparts with limited observing time, using 475 simulated gravitational wave events. Our results show a significant improvement in observing efficiency when compared with a naïve strategy of covering the entire localisation above some confidence threshold, even when achieving the same total probability covered.